Other
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.1502d&link_type=abstract
American Astronomical Society Meeting 210, #15.02; Bulletin of the American Astronomical Society, Vol. 39, p.113
Other
Scientific paper
The spectral mapping of Cassiopeia A with Spitzer has allowed us to use Doppler measurements to construct a 3-D model of the remnant structure. Combined with Doppler measurements from X-ray spectra and the locations of optical ejecta beyond the forward shock, we have gained new insights into the explosion that caused Cas A. The structure of Cas A can be characterized into "holes", "rings", and "jets". The holes refer to gaps between the front and back surfaces of the unshocked infrared ejecta that occur mostly in the plane of the sky. The shocked IR ejecta and the Si-rich X-ray ejecta form ring-like structures that line the holes in the unshocked ejecta. The well-known northeast and southwest jets extend through two of the holes in the unshocked ejecta. The Fe-rich X-ray ejecta has a different distribution from the other ejecta in that it is oriented approximately 90 degrees from the jet axis. The Fe-rich X-ray ejecta can be described as forming two jets that also extend through holes in the unshocked ejecta. The outer optical ejecta beyond the forward shock appears mostly in the plane of the sky and is certainly associated with the holes in the unshocked ejecta. Taken together, these clues indicate a series of blow-outs or jets in the plane of the sky where the highest velocity ejecta are found. The distribution of the Fe-rich ejecta provides a tidy explanation for the offset of the point source from the expansion center of the remnant and challenges the idea of overturning in the ejecta layers.
We would like to thank J. Lazendic and D. Dewey for their HETG Doppler data and M. Stage and G. Allen for their ACIS Ms Doppler data.
DeLaney Tracey
Ennis Jessica
Gomez Haley
Kozasa Takashi
Reach William
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